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GLAST Observations of Supernova Remnants and Pulsar Wind Nebulae Bryan Gaensler

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GLAST Observations of Supernova Remnants and Pulsar Wind Nebulae Bryan Gaensler NASA / ESA / J. Hester / A. Loll / ASU GLAST Observations of Supernova Remnants and Pulsar Wind Nebulae Bryan Gaensler The University of Sydney / Harvard-Smithsonian Center for Astrophysics Introduction • Supernova remnants (SNRs) & pulsar wind nebulae (PWNe) - broadband synchrotron emitters → shock acceleration of electrons to above ~1014 eV → are ions accelerated also? origin of cosmic rays up to “the knee”? - accelerated particles propagated via turbulence, winds, jets - emission traces interaction with surrounding gas - nearby laboratory for understanding AGN, µ-QSOs, clusters, GRBs • GLAST + (radio ⇔ TeV): direct measure of acceleration sites, mechanisms radio optical X-rays Crab Nebula (Hester et al. 2002) PSR B1509-58 (X-rays; Slane et al. 2006) SNR 3C 391 (radio; Moffett & Reynolds 1994) Particle Acceleration in SNRs • Emerging class of young SNRs emitting synchrotron X-rays - e.g., SN 1006, G347.3-0.5, Vela Jr., G330.2+1.0, RCW 86 - direct evidence of electron acceleration up to ~50-100 TeV (Koyama et al. 1995, 1997; Slane et al. 1999, 2001; Vink et al. 2006; Torii et al. 2006) • G347.3-0.5 & Vela Jr.: now seen at E > 100 GeV (Muraishi et al. 2000; Aharonian et al. 2004, 2005; Katagiri et al. 2005) SN 1006 (X-rays; NASA/CXC/ G347.3-0.5 (TeV; Aharonian et al. 2006) Vela Jr. (TeV; Aharonian et al. 2005) Rutgers/J.Hughes et al.) What Particles Are TeV Emitters? • π0 decay from p-p collisions GLAST (π0) HESS (e.g., Enomoto et al. 2002; Aharonian et al. 2006) - would be direct evidence for proton acceleration to > 10 TeV • Inverse Compton (IC) emission GLAST (IC) (e.g., Reimer & Pohl 2002; Lazendic et al. 2004) - - Synch. e scatter CMB, starlight, dust IR IC fit to G347.3-0.5 (Aharonian et al. 2006) • Spectroscopy can distinguish between p+ & e- - Cerenkov sees only high-energy tail LAT spectrum of G347.3-0.5 (Stefan Funk) - GLAST will measure overall shape • γ-ray imaging resolves acceleration sites - π0 decay should trace thermal X-rays - IC should trace non-thermal radio/X-rays • GLAST targets: - SNRs with synch. X-rays / TeV (e.g., RCW 86) - SNRs interacting with molec. clouds (e.g., W28) G347.3-0.5 (TeV, X-rays; Aharonian et al. 2004) Probes of SNR Environments I ( n M t e • For inverse Compton emission, o r s s k t e a l l l -rays probe photon field γ e a n r k r o a (Helfand et al. 2005; Porter et al. 2006) d e i t a t R = 0 kpc a i l o 0 . R = 3 kpc n • For π decay, γ-rays probe 2 0 R = 4 kpc f i 0 e 6 R = 7 kpc l d ambient density ) • Broadband fitting from radio to VHE γ-rays gives age, explosion energy, magnetic field, shock efficiency, Emax,e-, Emax,p+, etc. G 3 GLAST 4 7 . 3 - 0 . 5 ( E l l i s o n e t a l . 2 0 0 1 ) How Do Pulsars Accelerate Particles? • Theory says unshocked wind has γ ~ 106 • X-ray & γ-ray synchrotron emission in PWNe - termination shock accelerates particles to γ > 109 • GLAST bandpass needed to measure synch. roll-off - knowing γmax as fn. of pulsar parameters constrains mechanism GLAST Crab Nebula PWN around PSR B1509-58 Synchrotron spectrum of Crab (Chandra; Weisskopf et al. 2000) (INTEGRAL; Forot et al. 2006) (Atoyan & Aharonian 1996) Variability in Gamma-Ray PWNe • Gamma-ray emission from PWNe is variable, δt ~ months (de Jager et al. 1996; McLaughlin et al. 1996; Roberts et al. 2001; Ling & Wheaton 2003) • Synchrotron rather than IC • Simultaneous GLAST + Chandra - measurement of uncooled spectrum at acceleration site R - probe of flow as function of confinement conditions o b e r t s e t a l . ( 2 0 0 1 ) Crab Nebula (Weisskopf et al. 2000) The MouNseA (SGAae/CnsXleCr e/tA aSl.U 20/J0.4H)ester etB alla.ck Widow (NASA/CXC/M.Weiss) Inverse Compton Emission in PWNe • Several pulsar wind nebulae now seen with HESS - inverse Compton emission from CMB, starlight, IR from dust - Cerenkov detectors usually see high-energy tail - GLAST will see spectral peak + overlap with synchrotron IC Synchrotron GLAST PWN G0.9+0.1 (HESS/VLA; Aharonian et al. 2005) Broadband spectrum of G0.9.+0.1 (Aharonian et al. 2005) Inverse Compton in PWNe (cont.) • Synchrotron is convolution of N(E), B • IC depends on N(E), photon field • Spatial distribution of synch., IC - spatially resolved map of B - particle content, injection rate - σ = Efields/Eparticles • Pulsed IC from unshocked wind? (Ball & Kirk 1999; Bogovalov & Aharonian 2000) ) 0 0 0 2 n GLAST a i n a l o u r a b e h N A B1509-58 (Chandra; Slane et al. 2006) B1509-58 (HESS; Aharonian et al. 2005) b & a r v C o l a v o g o B ( Offset Gamma-Ray PWNe • HESS sees large TeV nebulae to one E > 2.5 TeV A h 0.8 < E < 2.5 TeV a r side of energetic pulsars o E < 0.8 TeV n i a - reverse shock from aspherical SNR? n e t a (Gaensler et al. 2003; Aharonian et al. 2005) l . ( 2 - systems need to expand rapidly, 0 0 PSR B1823-13 6 age ~ 5,000 - 20,000 years ) (e.g., de Jager & Venter 2005) • GLAST obs. of “Vela-like” pulsars B l o (Kramer et al. 2003) - ~25 sources known n d i n - nebulae will be v. large at E ~ 1 GeV e t a l . - morphology vs. E over five decades ( 2 0 0 → particle transport, magnetic fields, 1 ) diffusion, interaction with ISM/CSM Surveys & Discovery • > 1000 missing supernova remnants in Galaxy • Young pulsars without supernova remnants or pulsar wind nebulae - invisible in synchrotron if B is low ... but inverse Compton independent of B • Many new SNRs & PWNe seen w. GLAST, especially for |l| < 450 35 new SNRs in 1st Galactic quadrant (Brogan et al. 2006) 7000 year old pulsar B1610-50 (Stappers et al. 1999) NASA/CXC/SAO NASA / ESA / J. Hester / A. Loll /ASU Aurore Simonnet / Sonoma State y r a m m elp complete Galactic finally!) reveal sites & u h ( S spectra + multi-wavelength data will will will watch pulsars accelerate GLAST sample of SNRs & PWNe GLAST will tightly constrain evolution, environment, ambient photon field of SNRs & PWNe particles and magnetic fields in PWNe GLAST particles in real time GLAST will map distribution, evolutionary history, injection rate of GLAST products of particle acceleration in SNRs • • • • •.
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